About: VW Leonis Minoris

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VW Leo Minoris is a tight quadruple star system, located in the constellation of Leo Minor. With a peak combined apparent visual magnitude of 8.07, it is too faint to be seen with the naked eye. Parallax measurements give a distance estimate of approximately 370 light years from the Sun, and it is drifting further away with a radial velocity of +5 km/s. Hierarchy of orbits

Attributes	Values
rdf:type	Thing place dbo:Location schema:Place celestial body star
rdfs:label	VW Leonis Minoris (en)
rdfs:comment	VW Leo Minoris is a tight quadruple star system, located in the constellation of Leo Minor. With a peak combined apparent visual magnitude of 8.07, it is too faint to be seen with the naked eye. Parallax measurements give a distance estimate of approximately 370 light years from the Sun, and it is drifting further away with a radial velocity of +5 km/s. Hierarchy of orbits (en)
foaf:depiction
dcterms:subject	Durchmusterung objects F-type main-sequence stars G-type main-sequence stars Henry Draper Catalogue objects Hipparcos objects Leo Minor Multiple star systems Objects with variable star designations W Ursae Majoris variables
Wikipage page ID	66744111 (xsd:integer)
Wikipage revision ID	1094513166 (xsd:integer)
Link from a Wikipage to another Wikipage	Stellar classification Light curve Durchmusterung objects F-type main-sequence stars G-type main-sequence stars Henry Draper Catalogue objects Hipparcos objects Leo Minor Multiple star systems Objects with variable star designations Constellation Orbital plane Apsidal precession Leo Minor Light year Star Orbital period Stellar parallax Transiting Exoplanet Survey Satellite W Ursae Majoris variable G-type main-sequence star W Ursae Majoris variables Hipparcos Sun Eclipsing binary Apparent visual magnitude Orbital eccentricity Radial velocity Orbital inclination Variable star Common proper motion F-type main sequence star
reference	(en) – Contact (en) – Mutual (en) – Non-contact (en)
sameAs	VW Leonis Minoris VW Leonis Minoris
dbp:wikiPageUsesTemplate	dbt:Chart dbt:Chart/end dbt:Chart/start dbt:Convert dbt:Reflist dbt:Short_description dbt:Starbox_astrometry dbt:Starbox_begin dbt:Starbox_catalog dbt:Starbox_character dbt:Starbox_detail dbt:Starbox_end dbt:Starbox_image dbt:Starbox_observe dbt:Starbox_orbit dbt:Starbox_reference dbt:Stars_of_Leo_Minor dbt:Val dbt:DEC dbt:Odlist dbt:RA
thumbnail	wiki-commons:Special:FilePath/VWLMiLightCurve.png?width=300
absmag v	2.460000 (xsd:double)
appmag v	8.070000 (xsd:double)
class	F2V + G2V (en)
component	Component 1 (en) Component 2 (en)
constell	Leo Minor
eccentricity	0 (xsd:integer)
epoch	J2000.0 (en)
luminosity	8.730000 (xsd:double)
p error	0.104600 (xsd:double)
parallax	8.823800 (xsd:double)
prop mo dec	−4.764 (en)
prop mo ra	+12.304 (en)
variable	Suspected W UMa (en)
has abstract	VW Leo Minoris is a tight quadruple star system, located in the constellation of Leo Minor. With a peak combined apparent visual magnitude of 8.07, it is too faint to be seen with the naked eye. Parallax measurements give a distance estimate of approximately 370 light years from the Sun, and it is drifting further away with a radial velocity of +5 km/s. Hierarchy of orbits This system was found to be variable using observations with the Hipparcos satellite. It is classified as an A-type W Ursae Majoris eclipsing binary, where the two stars share a common envelope. The eclipse of the primary causes the magnitude of the system to drop to 8.45. These components (1 & 2) have an orbital period of 11.4611 hours and the orbital plane has an inclination of 72.4° to the line of sight from the Earth. They have a combined stellar classification of F2V, matching an F-type main sequence star. In 2006 an additional, detached binary component was discovered, making this a quadruple star system. This binary has an orbital period of 7.93 days, a mild eccentricity (ovalness) of 0.04, and it shows an apsidal precession with a period of 78.6±1.6 years. The components (3 & 4) have a combined stellar class of G2V, showing a match with a G-type main-sequence star. The two binaries (1–2 & 3–4) orbit each other with a period of 355 days and an eccentricity of 0.1. The plane of their orbit is close to coplanar (within 5°) with the orbital plane of the detached binary. This outer orbit appears stable, suggesting there is no additional outlying component to this system. The nearby ninth magnitude star HD 95606 (HIP 53969) shares a common proper motion with this system and may be loosely gravitationally bound. They likely all formed in the same protostellar cloud. (en)
prov:wasDerivedFrom	wikipedia-en:VW_Leonis_Minoris?oldid=1094513166&ns=0
page length (characters) of wiki page	10160 (xsd:nonNegativeInteger)
foaf:isPrimaryTopicOf	wikipedia-en:VW_Leonis_Minoris
is Link from a Wikipage to another Wikipage of	List of stars in Leo Minor

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